J/A+A/660/A78 LoTSS-DR2 sample overview release (Botteon+, 2022)
The Planck clusters in the LOFAR sky.
I. LoTSS-DR2: New detections and sample overview.
Botteon A., Shimwell T.W., Cassano R., Cuciti V., Zhang X., Bruno L.,
Camillini L., Natale R., Jones A., Gastaldello F., Simionescu A.,
Rossetti M., Akamatsu H., van Weeren R.J., Brunetti G., Brueggen M.,
Groeneveld C., Hoang D.N., Hardcastle M.J., Ignesti A., Di Gennaro G.,
Bonafede A., Drabent A., Roettgering H.J.A., Hoeft M., de Gasperin F.
<Astron. Astrophys. 660, A78 (2022)>
=2022A&A...660A..78B 2022A&A...660A..78B (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Radio continuum ; Clusters, galaxy ; Radio sources
Keywords: galaxies: clusters: general -
galaxies: clusters: intracluster medium - catalogs -
radiation mechanisms: nonthermal - radiation mechanisms: thermal -
Abstract:
Relativistic electrons and magnetic fields permeate the intra-cluster
medium (ICM) and manifest themselves as diffuse sources of synchrotron
emission observable at radio wavelengths, namely radio halos and radio
relics. Although there is broad consensus that the formation of these
sources is connected to turbulence and shocks in the ICM, the details
of the required particle acceleration, the strength and morphology of
the magnetic field in the cluster volume, and the influence of other
sources of high-energy particles are poorly known. Sufficiently large
samples of radio halos and relics, which would allow us to examine the
variation among the source population and pinpoint their commonalities
and differences, are still missing. At present, due to the physical
properties of the sources and the capabilities of existing facilities,
large numbers of these sources are easiest to detect at low radio
frequencies, where they shine brightly. We examined the low-frequency
radio emission from all 309 clusters in the second catalog of Planck
Sunyaev Zel'dovich detected sources that lie within the 5634 deg2
covered by the Second Data Release of the LOFAR Two-meter Sky Survey
(LoTSS-DR2). We produced LOFAR images at different resolutions, with
and without discrete sources subtracted, and created overlays with
optical and X-ray images before classifying the diffuse sources in the
ICM, guided by a decision tree. Overall, we found 83 clusters that
host a radio halo and 26 that host one or more radio relics (including
candidates). About half of them are new discoveries. The detection
rate of clusters that host a radio halo and one or more relics in our
sample is 30±11% and 10±6%, respectively. Extrapolating these
numbers, we anticipate that once LoTSS covers the entire northern sky
it will provide the detection of 251±92 clusters that host a halo
and 83±50 clusters that host at least one relic from Planck
clusters alone. All images and results produced in this work are
publicly available via the project website.
Description:
The attached tables collect the results from the analysis of the
galaxy clusters covered by the second LOFAR Two-metre Sky Survey Data
Release (LoTSS-DR2) that belong to the second Planck catalog of
Sunyaev-Zel'dovich sources (PSZ2). Tables contain the main properties
of the full sample of galaxy clusters with the classification of the
radio sources, the X-ray morphological parameters of the intra-cluster
medium obtained with Chandra and XMM-Newton observations, and the
properties derived for the radio halos and relics in the sample. With
309 objects, the LoTSS-DR2/PSZ2 sample represents the largest
statistical sample of galaxy clusters observed with highly sensitive
low frequency observations that has been ever used to search for and
study diffuse synchrotron emission in the intra-cluster medium. The
results of this work are presented in the series of papers entitled
"The Planck clusters in the LOFAR sky".
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
fsamp.dat 808 309 Full sample of PSZ2 clusters in LoTSS-DR2
(table A1)
cwsamp.dat 61 150 Subsample of galaxy clusters with
Chandra/XMM-Newton data available for which we
computed the X-ray morphological parameters
(table A2)
rhsamp.dat 177 73 Sample of radio halos and candidate radio halos
found in this work (table A3)
rrsamp.dat 115 35 Sample of radio relics and candidate radio
relics found in this work (table A4)
arhsamp.dat 113 10 Sample of radio halos and candidate radio halos
that were classified with an asterisk because
of their low significance (table C1)
--------------------------------------------------------------------------------
See also:
https://lofar-surveys.org/planck_dr2.html :
The Planck clusters in the LOFAR sky project website
Byte-by-byte Description of file: fsamp.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Name Name of the source, PSZ2 GLLL.ll+BB.bb
(Name)
20- 27 F8.4 deg RAdeg Right ascension (J2000) (RA)
29- 35 F7.4 deg DEdeg Declination (J2000) (DEC)
37-674 A638 --- ANames Alternative names (Alternative names)
676-680 F5.3 --- z ?=- Redshift of the source (z)
682-686 F5.2 10+14Msun M500 ?=- Mass of the source(M500)
688-691 F4.2 10+14Msun e_M500 ?=- Error on Mass of the source(M500_err)
693-696 I4 kpc R500 ?=- Radius of the source(R500)
698-699 I2 kpc e_R500 ?=- Error on Radius of the source (R500_err)
701-702 I2 --- Qual Quality of the reference LOFAR radio image
(Image quality)
704-709 F6.3 mJy/beam rms Noise of the reference LOFAR radio image
(rms)
711-718 A8 --- Class Classification of the radio emission
(Classification)
720-722 A3 --- X-ray [C/X -] Presence of pointed X-ray data
(X-ray) (1)
724-808 A85 --- Com Comments and remarks on this entry (Comment)
--------------------------------------------------------------------------------
Note (1): 'C' indicates Chandra and 'X' indicates XMM-Newton.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: cwsamp.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Name Name of source, PSZ2 GLLL.ll+BB.bb (Name)
20- 21 A2 --- Subcluster Position of the subcluster (Subcluster) (1)
23- 28 F6.4 --- c Concentration parameter (c)
30- 36 F7.5 --- e_c Error on the concentration parameter (c_err)
38- 44 F7.5 --- w Centroid shift (w)
46- 57 E12.6 --- e_w Error on the centroid shift (w_err)
59- 61 A3 --- X-ray [C+X ] X-ray data used to compute the
morphological parameters (X-ray) (2)
--------------------------------------------------------------------------------
Note (1): Positions as E, E1, E2, EN, ES, N, S, W, W1 or W2.
Note (2): 'C' indicates Chandra and 'X' indicates XMM-Newton.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: rhsamp.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Name Name of source, PSZ2 GLLL.ll+BB.bb (Name)
20- 25 F6.2 mJy S150 ?=- Flux density of the radio halo at
150MHz integrated within the 2sigma region
(S150 (2sigma))
27- 31 F5.2 mJy e_S150 ?=- Error on the flux density of the radio
halo at 150MHz integrated within the
2sigma region (S150_err (2sigma))
33- 38 F6.2 mJy S150f ?=- Flux density of the radio halo at
150MHz obtained from the surface
brightness profile fitting (S150 (fit))
40- 44 F5.2 mJy e_S150f ?=- Error on the flux density of the radio
halo at 150MHz obtained from the surface
brightness profile fitting
(S150_err (fit))
46- 57 E12.6 W/Hz P150 ?=- k-corrected radio power of the radio
halo at 150MHz (P150)
59- 70 E12.6 W/Hz e_P150 ?=- Error on the k-corrected radio power of
the radio halo at 150 MHz (P150_err)
72- 76 F5.2 uJy/arcsec2 I0 ?=- Best-fit central brightness (I0)
78- 81 F4.2 uJy/arcsec2 e_I0 ?=- Error on the best-fit central
brightness (I0_err)
83- 87 F5.1 kpc r1 ?=- Best-fit first e-folding radius (r1)
89- 92 F4.1 kpc e_r1 ?=- Error on the best-fit first e-folding
radius (r1_err)
94- 98 F5.1 kpc r2 ?=- Best-fit second e-folding radius (r2)
100-102 F3.1 kpc e_r2 ?=- Error on the best-fit second e-folding
radius (r2_err)
104-118 A15 --- Model Model used to fit the radio halo (Model)
120-125 F6.2 --- SNR ?=- Signal-to-noise ratio of the fit (SNR)
127-131 F5.3 mJy/beam rms ?=- Noise of the LOFAR radio image used for
the fit (rms)
133-137 F5.2 --- chi2r ?=- Reduced chi2 of the fit (chi2red)
139-177 A39 --- Com Comments and remarks on this entry
(Comment)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: rrsamp.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Name Name of source, PSZ2 GLLL.ll+BB.bb (Name)
20- 21 A2 --- Pos Position of the radio relic with respect to
the cluster (Position) (1)
23- 30 F8.4 deg RAdeg Radio relic right ascension (J2000) (RA_RR)
32- 38 F7.4 deg DEdeg Radio relic declination (J2000) (DEC_RR)
40- 45 F6.2 mJy S150 Flux density of the radio relic at 150MHz
(S150)
47- 51 F5.2 mJy e_S150 Error on the flux density of the radio relic
at 150MHz (S150_err)
53- 64 E12.6 W/Hz P150 k-corrected radio power of the radio relic
at 150MHz (P150)
66- 77 E12.6 W/Hz e_P150 Error on the k-corrected radio power of the
radio relic at 150MHz (P150_err)
79- 82 I4 kpc LLS Largest-linear size of the radio relic (LLS)
84- 85 I2 kpc e_LLS Error on the largest-linear size of the
radio relic (LLS_err)
87- 89 I3 kpc Width Width of the radio relic (Width)
91- 93 I3 kpc e_Width Error on the width of the radio relic
(Width_err)
95- 98 I4 uJy/beam SBavg Average surface brightness of the radio relic
(Average SB)
100-103 I4 kpc DRR-c ?=- Distance between the radio relic and X-ray
centroid of the cluster (D_RR-c)
105-107 I3 kpc e_DRR-c ?=- Error on the distance between the radio
relic and X-ray centroid of the cluster
(DRR-cerr)
109-112 I4 kpc DRR-RR ?=- Distance between double radio relics
(D_RR-RR)
114-115 I2 kpc e_DRR-RR ?=- Error on the distance between double
radio relics (DRR-RRerr)
--------------------------------------------------------------------------------
Note (1): Positions are E, N, N1, N2, S or W.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: arhsamp.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Name Name of the source, PSZ2 GLLL.ll+BB.bb
(Name)
20- 24 F5.2 mJy S150 Flux density of the radio halo at 150MHz
integrated within the 2sigma region
(S150 (2sigma))
26- 29 F4.2 mJy e_S150 Error on the flux density of the radio
halo at 150MHz integrated within the
2sigma region (S150_err (2sigma))
31- 35 F5.2 mJy S150f Flux density of the radio halo at 150MHz
obtained from the surface brightness
profile fitting (S150 (fit))
37- 41 F5.2 mJy e_S150f Error on the flux density of the radio
halo at 150MHz obtained from the surface
brightness profile fitting
(S150_err (fit))
43- 54 E12.6 W/Hz P150 k-corrected radio power of the radio halo
at 150MHz (P150)
56- 67 E12.6 W/Hz e_P150 Error on the k-corrected radio power of
the radio halo at 150MHz (P150_err)
69- 72 F4.2 uJy/arcsec2 I0 Best-fit central brightness (I0)
74- 77 F4.2 uJy/arcsec2 e_I0 Error on the best-fit central brightness
(I0_err)
79- 83 F5.1 kpc r1 Best-fit e-folding radius (r1)
85- 89 F5.1 kpc e_r1 Error on the best-fit e-folding radius
(r1_err)
91- 96 A6 --- Model [circle] Model used to fit the radio halo
(Model)
98-102 F5.2 --- SNR Signal-to-noise ratio of the fit (SNR)
104-108 F5.3 mJy/beam rms Noise of the LOFAR radio image used for
the fit (rms)
110-113 F4.2 --- chi2red Reduced chi2 of the fit (chi2red)
--------------------------------------------------------------------------------
Acknowledgements:
Andrea Botteon, botteon(at)strw.leidenuniv.nl
(End) Patricia Vannier [CDS] 14-Feb-2022